Modeling Emission Lines from Dwarf Novae in Quiescence

Details Modeling Emission Lines from Dwarf Novae in Quiescence Modeling Emission Lines from Dwarf Novae in Quiescence

Jan 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996apj...457..363k&link_type=abstract

Astrophysical Journal v.457, p.363

Astronomy and Astrophysics

Astronomy

16

Accretion, Accretion Disks, Line: Formation, Stars: Novae, Cataclysmic Variables, X-Rays: Stars

Scientific paper

For cataclysmic variables with disk accretion, it is plausible that X-rays/extreme-ultraviolet (EUV) radiation as a result of accretion can back-illuminate the accretion disk. Such illumination will photoionize and heat up the disk to form a temperature-inverted layer in which emission lines can form. We make self-consistent, non-LTE calculations of the vertical structure, ionization, ion level populations, and the emitted spectrum for such photoionized layers. We compare the emerging emission-line spectra with the observations of dwarf novae in quiescence from lUE. We show that a strong soft X-ray/EUV component is necessary to explain the observed UV line strengths. We also explore the possibility of UV line production from disks heated only by viscous dissipation.

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